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31.
32.
应用联合变换相关器的成像制导系统 总被引:1,自引:0,他引:1
提出了一种光电混合的成像制导系统,它采用光学联合变换相关器作为其主要的图像识别单元,利用计算机对识别结果进行判决和显示,并发出跟踪信号给导引头,从而实现制导。联合变换相关器是对光学图像信号进行并行处理的器件,实时识别性能强,精度高。此成像制导系统克服了传统的红外制导系统易受外界因素影响,实时处理能力差,误判率较高的缺点,具有并行处理速度快、信息吞吐量大、体积小等优点,应用前景广阔。 相似文献
33.
红外型空空导弹智能制导律研究 总被引:1,自引:0,他引:1
本文论述了红外型空空导弹应用智能控制的理论基础及结构特点,以多级智能控制的框架和机理设计出以比例导引为主、智能控制为辅的变指令智能制导律,并编制计算机软件以数字仿真的形式验证变指令智能制导规律的有效性和可行性 相似文献
34.
远程导引可行飞行方案寻求算法研究 总被引:4,自引:1,他引:4
提出了一种寻求远程导引可行飞行方案的算法,能够满足远程导引对测控、日照、燃料和时间等各方面的要求;重点论述了Lambert一次变轨方案,给出了算法的具体步骤和主要模块的实现方法;最后给出了一个算例,说明算法是切实可行的。 相似文献
35.
阐述了惯导测试设备的作用、种类,介绍了其典型结构及基本精度指标的概念。说明了惯导测试设备的发展趋势;总体布局向卧式发展;轴系结构向有源磁悬浮发展;台体向复合材料球形壳体发展;输电装置向滚环发展;分度元件采用高精度的感应同步器。列举了检定技术的实例,说明了其发展方向:不断提高检定精度;开展动态检定;改善测量设备对三轴空间位置的适应性。此外,管理上要制度化,名词术语与数据处理要标准化,设计与检定要相协调。 相似文献
36.
姜玉宪 《北京航空航天大学学报》1989,(3):87-95
本文提出一种能够实现导弹对活动目标全方位攻击的基本原理,并讨论了工程上实现的途径。通过平面及空间导引弹道仿真,初步证明了它的正确性及可实现性。 相似文献
37.
反舰导弹变系数修正比例导引研究 总被引:4,自引:2,他引:4
针对超音速反舰导弹自导段控制的特点,对比分析了两种典型的非线性导引规律即反馈线性化(FLGL)导引律和逆向接近导引律的优缺点,提出了一种称为变系数修正比例导引的方法,通过对其全弹道仿真结果的分析,说明所提出的导引规律是正确的,具有良好的应用效果。 相似文献
38.
S. M. Krimigis D. G. Mitchell D. C. Hamilton S. Livi J. Dandouras S. Jaskulek T. P. Armstrong J. D. Boldt A. F. Cheng G. Gloeckler J. R. Hayes K. C. Hsieh W.-H. Ip E. P. Keath E. Kirsch N. Krupp L. J. Lanzerotti R. Lundgren B. H. Mauk R. W. McEntire E. C. Roelof C. E. Schlemm B. E. Tossman B. Wilken D. J. Williams 《Space Science Reviews》2004,114(1-4):233-329
The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R
S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm2 sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm2 sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm2 sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm2 sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R
S every 2–3 h (every ∼10 min from ∼20 R
S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date. 相似文献
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40.
主动段扰动引力是引起弹道导弹制导方法误差的主要因素。因此,要提高导弹的制导精度,就必须能够在弹上实时计算扰动引力。但现有方法在计算快速性和存储量之间无法得到有效协调。为此,把广义延拓逼近思想引入有限元逼近方法中,将插值单元周围节点的信息也包含到单元内一点扰动引力的计算当中,建立了一种新的数学模型。对所选发射空域,在发射坐标系中进行了直角坐标划分。计算结果表明,这种方法能够更加精确地逼近弹道导弹主动段的扰动引力,在600 km×250 km×6 km的主动段飞行区域内,只需要保存60个节点数据,就能使由逼近误差导致的落点偏差小于10 m,是一般有限元逼近方法精度的4倍以上。 相似文献